Analysis of the orbital evolution of exoplanets
| Autor: | R. Vilhena de Moraes, J. P. S. Carvalho, D. C. Mourão, Antonio F. B. A. Prado, Othon C. Winter |
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| Přispěvatelé: | Universidade Federal do Recôcavo da Bahia, Universidade Federal de São Paulo (UNIFESP), INPE, Universidade Estadual Paulista (Unesp) |
| Rok vydání: | 2015 |
| Předmět: |
Physics
Orbital elements 010504 meteorology & atmospheric sciences Clearing the neighbourhood Applied Mathematics Retrograde motion Astronomy Astrophysics Planetary system 01 natural sciences Exoplanet Planetary systems Computational Mathematics Astrodynamics Planet Sub-Earth Stellar dynamics Exoplanets and third-body perturbation 0103 physical sciences Astrophysics::Solar and Stellar Astrophysics Astrophysics::Earth and Planetary Astrophysics 010303 astronomy & astrophysics 0105 earth and related environmental sciences |
| Zdroj: | Scopus Repositório Institucional da UNESP Universidade Estadual Paulista (UNESP) instacron:UNESP |
| ISSN: | 1807-0302 0101-8205 |
| DOI: | 10.1007/s40314-015-0270-z |
| Popis: | Made available in DSpace on 2018-12-11T17:29:44Z (GMT). No. of bitstreams: 0 Previous issue date: 2016-10-01 An exoplanet, or extrasolar planet, is a planet that does not orbit the Sun, but is around a different star, stellar remnant, or brown dwarf. Up to now, about 1900 exoplanets were discovered. To better understand the dynamics of these exoplanets, a study with respect to possible collisions of the planet with the central star is shown here. We present an expanded model in a small parameter that takes into account up to the fifth order to analyze the effect of this potential in the orbital elements of the extrasolar planet. Numerical simulations were also performed using the N-body simulations, using the software Mercury, to compare the results with the ones obtained by the analytical model. The numerical simulations are presented in two stages: one considering the celestial bodies as point masses and the other one taking into account their dimensions. This analysis showed that the planet collided with the central star in the moment of the first inversion for orbits with high inclinations in various situations. The results of the simulations of the equations developed in this study are consistent with the N-body numerical simulations. We analyze also the flip of the inclination taking into account the coupling of the perturbations of the third body, effect due to the precession of periastron and the tide effect. In general, we find that such perturbations combined delay the time of first inversion, but do not keep the planet in a prograde or retrograde orbit. UFRB Centro de Ciência e Tecnologia em Energia e Sustentabilidade Universidade Federal do Recôcavo da Bahia UNIFESP Instituto de Ciência e Tecnologia Universidade Federal de São Paulo Division of Space Mechanics and Control INPE UNESP Univ Estadual Paulista UNESP Univ Estadual Paulista |
| Databáze: | OpenAIRE |
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